Building upon the success of this first study, a NIKA2 Open Time (OT) program aiming at mapping the SZ signal of 5 MOO-X/SZ clusters already observed by Chandra as well as a Large Program (LP) dedicated to the Chandra observation of 4 MOO-X/SZ clusters already observed by MUSTANG-2 have been accepted. The NIKA2 OT observations were completed in March 2021 and the Chandra LP observations are still on-going. In Fig. REF , we present preliminary maps of 4 MOO-X/SZ clusters obtained in SZ (top) and X-ray (bottom). The first SZ map on the left has been obtained with MUSTANG-2 at 90 GHz and the three other maps present NIKA2 data at 150 GHz [1]}. The SZ signal is detected at \(>7\sigma \)  in all maps. We observe similar cluster morphologies in SZ and X-ray and we identify ICM disturbances in each cluster. For example, MOO J0319\(-\) 0025 at \(z=1.19\)  displays a clear bi-modal morphology while MOO J1014\(+\) 0038 at \(z=1.23\)  presents ICM substructures in the south-west region. These preliminary results tend to confirm our expectation that ICM disturbances due to merging events are more frequently observed at \(z > 1\)  than in low redshift cluster samples such as REXCESS [2]} or CCCP [3]}. Based on the tools that we developed for the analysis of MOO J1142\(+\) 1527, we are currently analyzing jointly our X-ray and SZ data sets in order to provide a detailed characterization of the ICM properties in a sample of \(z>0.9\)  clusters for the first time. In particular, we are producing ICM temperature and entropy maps that we cross correlate with the galaxy distribution of each cluster in order to understand their merger dynamics. We also aim at exploring the connection between the ICM thermodynamic properties of all MOO-X/SZ clusters and the potential radio emission of the brightest cluster galaxy in order to better understand AGN feedback at high redshift. The analysis of the spectroscopic information embedded within our Chandra data using prior information on the ICM temperature obtained from the joint X-ray / SZ analysis will allow us to constrain the metallicity content of these cluster in order to understand metal enrichment at high redshift. Finally, the hydrostatic masses obtained from the estimated density and pressure profiles of these clusters will be compared to the richness-derived masses obtained with Spitzer in order to unveil potential systematic effects on the mass-richness scaling relation derived at high redshift. The full characterization of the MOO-X/SZ sample will thus provide valuable information that will pave the way to an in-depth understanding of cluster formation at \(z > 1\)  and to precise cluster cosmological constraints from the forthcoming optical/IR surveys such as Euclid [4]} and Rubin-LSST [5]}.
